Skip to main content

Research Repository

Advanced Search

On the nature of superoutbursts in dwarf novae

Truss, M.R.; Murray, J.R.; Wynn, G.A.

Authors

M.R. Truss

J.R. Murray

G.A. Wynn



Abstract

We present the first detailed hydrodynamic simulation of a superoutburst to incorporate the full tidal potential of a binary system. A two-dimensional smoothed particle hydrodynamics code is used to simulate a superoutburst in a binary with the parameters of the SU UMa system Z Chamaeleontis. The simulated light curves shows all the features observed in such systems. Analysis of the mass flux through the disc and the growth rate of the superhumps and disc eccentricity show that the superoutburst–superhump phenomenon is a direct result of tidal instability. No enhanced mass transfer from the secondary is required to initiate or sustain these phenomena. Comparisons of superoutbursts with normal outbursts are made and we show that the model can be reconciled with the behaviour of U Geminorum-type dwarf novae, which show no superoutbursts.

Citation

Truss, M., Murray, J., & Wynn, G. (2001). On the nature of superoutbursts in dwarf novae. Monthly Notices of the Royal Astronomical Society, 324(1), L1-L5. https://doi.org/10.1046/j.1365-8711.2001.04535.x

Journal Article Type Article
Publication Date 2001-06
Deposit Date Apr 28, 2008
Publicly Available Date Apr 28, 2008
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 324
Issue 1
Pages L1-L5
DOI https://doi.org/10.1046/j.1365-8711.2001.04535.x
Keywords Accretion discs, Instabilities, Binaries, Novae, Cataclysmic variables.

Files




You might also like



Downloadable Citations